BaymPethickSutherland equation of state. More...
#include <eos_crust.h>
Public Types  
typedef boost::numeric::ublas::vector< double >  ubvector 
Public Member Functions  
virtual int  calc_density (double barn, thermo &th, int &Z, int &A) 
Calculate the equation of state as a function of the baryon number density barn . More...  
virtual int  calc_pressure (thermo &th, double &barn, int &Z, int &A) 
Calculate the equation of state as a function of the pressure. More...  
virtual double  lattice_energy (int Z) 
The electron lattice energy.  
virtual const fermion &  get_electron () 
Get a pointer to the electron.  
virtual double  mass_formula (int Z, int A) 
The mass formula. More...  
virtual const char *  type () 
Return string denoting type ("eos_crust")  
int  set_mass_formula (nucmass &nm) 
Set the nuclear mass formula to be used.  
int  calc_density_fixedA (double barn, thermo &th, int &Z, int A) 
Compute the ground state assuming a fixed atomic number.  
Public Member Functions inherited from o2scl::eos_base  
virtual void  set_thermo (thermo &th) 
Set class thermo object.  
virtual const thermo &  get_thermo () 
Get class thermo object.  
Public Attributes  
nucmass_semi_empirical  def_mass 
Default mass formula.  
fermion  e 
The electron thermodynamics. More...  
Public Attributes inherited from o2scl::eos_base  
thermo  def_thermo 
The default thermo object.  
Protected Member Functions  
virtual int  eq274 (size_t nv, const ubvector &nx, ubvector &ny, int &Zt) 
Solve Equation 2.7.4 for a given pressure.  
double  gibbs (int Z, int A) 
The Gibbs free energy.  
double  energy (double barn, int Z, int A) 
The energy density.  
Protected Attributes  
fermion_zerot  fzt 
Zerotemperature thermodynamics for the electrons.  
mroot_hybrids< mm_funct11 >  gs 
A solver to solve Eq. 2.7.4.  
nucmass *  nmp 
The nuclear mass formula.  
Protected Attributes inherited from o2scl::eos_base  
thermo *  eos_thermo 
A pointer to the thermo object.  
This calculates the equation of state of electrons and nuclei using the approach of Baym71tg (based on the discussion in Shapiro83) between about and . Below these densities, more complex Coulomb corrections need to be considered, and above these densities, neutron drip is important.
The default mass formula is semiempirical
where
if the nucleus is oddodd (plus sign) or eveneven (minus sign) and is zero for oddeven and evenodd nuclei. The nuclei are assumed not to contribute to the pressure. The electronic contribution to the pressure is assumed to be equal to the Fermi gas contribution plus a "lattice" contribution
This is Eq. 2.7.2 in Shapiro83. The rest mass energy of the nucleons is included in the energy density.
The original results from Baym71tg are stored as a table in file data/o2scl/bps.eos
. The testing code for this class compares the calculations to the table and matches to within .2 percent for the energy density and 9 percent for the pressure (for a fixed baryon number density).
Can the pressure be made to match more closely?
Convert to a o2scl::eos_had_base object and offer an associated interface?
Definition at line 84 of file eos_crust.h.

virtual 
This calculates the equation of state as a function of the baryon number density in , returning the representative nucleus with proton number Z
and atomic number A
. The pressure and energy density are returned in th
in .

virtual 
This calculates the equation of state as a function of the pressure, returning the representative nucleus with proton number Z
and atomic number A
and the baryon number density barn
in . The energy density is also returned in in th
.

virtual 
The nuclear mass without the contribution of the rest mass of the electrons. The electron rest mass energy is included in the electron thermodynamics elsewhere.
fermion o2scl::eos_crust::e 
Definition at line 151 of file eos_crust.h.
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